A ROSAT HRI study of the interaction of the X-ray-emitting gas and radio lobes of NGC 1275

Böehringer, H.; Voges, W.; Fabian, A. C.; Edge, A. C.; Neumann, D. M.

doi:10.1093/mnras/264.1.l25

Cited by 470 publications

(427 citation statements)

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“…Over the years the AGN feedback mechanism, mostly by jet-inflated bubbles, has been solidified (e.g., Dong et al 2010;O'Sullivan et al 2011;Farage et al 2012;Gaspari et al 2012a,b;Birzan et al 2011;Gitti et al 2012;Pfrommer 2013). Key to the establishment of the AGN-JFM in cooling flows are the many observations of X-ray deficient bubbles (e.g., Boehringer et al 1993;Fabian et al 2000;McNamara et al 2001;Heinz et al 2002;Forman et al 2007;Wise et al 2007;Baldi et al 2009;David et al 2009;Gastaldello et al 2009;Gitti et al 2010;Blanton et al 2011;David et al 2011;Machacek et al 2011;Randall et al 2011;Doria et al 2012;Pandge et al 2012;Hlavacek-Larrondo et al 2015). Many of these X-ray bipolar structures resemble visible bipolar structures observed in bipolar PNe (see Figs.…”

Section: Jet-inflated Bubblesmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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Section: Jet-inflated Bubblesmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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“…(1) Boehringer et al (1993); Heinz, Reynolds, & Begelman (1998);Churazov et al (2000); Fabian et al (2000) (2) estimated from the images, see Fig. 6 (3) …”

Section: Observed Simulatedmentioning

confidence: 99%

The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster

Zhuravleva

Churazov

Arévalo

et al. 2016

Mon. Not. R. Astron. Soc.

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Cores of relaxed galaxy clusters are often disturbed by AGN. Their Chandra observations revealed a wealth of structures induced by shocks, subsonic gas motions, bubbles of relativistic plasma, etc. In this paper, we determine the nature and energy content of gas fluctuations in the Perseus core by probing statistical properties of emissivity fluctuations imprinted in the soft-and hard-band X-ray images. About 80 per cent of the total variance of perturbations on ∼ 8 − 70 kpc scales in the inner region have an isobaric nature, i.e., are consistent with slow displacements of the gas in pressure equilibrium with ambient medium. Observed variance translates to the ratio of nonthermal to thermal energy of ∼ 13 per cent. In the region dominated by weak "ripples", about half of the total variance is also associated with isobaric perturbations on scales a few tens of kpc. If these isobaric perturbations are induced by buoyantly rising bubbles, then these results suggest that most of the AGN-injected energy should first go into bubbles rather than into shocks. Using simulations of a shock propagating through the Perseus atmosphere, we found that models reproducing the observed features of a central shock have more than 50 per cent of the AGN-injected energy associated with the bubble enthalpy and only about 20 per cent is carried away with the shock. Such energy partition is consistent with the AGN-feedback model, mediated by bubbles of relativistic plasma, and supports the importance of turbulence in the balance between gas heating and radiative cooling.

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“…Various works propose that the observed radio lobes of active galactic nuclei, like Hydra A, form cavities in the cluster atmosphere, see e.g. Böhringer et al (1993), Enßlin (1999), McNamara et al (2000), Fabian et al (2000), and David et al (2001). In these cavities the polarised radio light is produced, but n e (x) is presumably so low that no significant Faraday rotation is expected to occur there.…”

Section: Window Functionmentioning

confidence: 99%

Magnetic power spectra from Faraday rotation maps

Kuchar

Enßlin

2011

A&A

103

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We develop a novel maximum-a-posteriori method to measure magnetic power spectra from Faraday rotation data and implement it in the REALMAF code. A sophisticated model for the magnetic autocorrelation in real space permits us to alleviate previously required simplifying assumptions in the processing. We also introduce a way to treat the divergence relation of the magnetic field with a multiplicative factor in Fourier space, with which we can model the magnetic autocorrelation as a spherically symmetric function. Applied to the dataset of Hydra A north, we find a power law power spectrum on spatial scales between 0.3 kpc and 8 kpc, with no visible turnover at large scales within this range and a spectral index consistent with a Kolmogorov-like power law regime. The magnetic field strength profile seems to follow the electron density profile with an index α = 1. A variation of α from 0.5 to 1.5 would lead to a spectral index between 1.55 and 2.05. The extrapolated magnetic field strength in the cluster centre highly depends on the assumed projection angle of the jet. For an angle of 45 • we derive extrapolated 36 μG in the centre and directly probed 16 μG at 50 kpc radius.

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A ROSAT HRI study of the interaction of the X-ray-emitting gas and radio lobes of NGC 1275

Cited by 470 publications

References 0 publications

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster

Magnetic power spectra from Faraday rotation maps

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